The subphotospheric structure of a sunspot

Details The subphotospheric structure of a sunspot The subphotospheric structure of a sunspot

Jul 2009

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009arep...53..675s&link_type=abstract

Astronomy Reports, Volume 53, Issue 7, pp.675-683

Astronomy and Astrophysics

Astronomy

1

96.60.Qd, 96.60.Hv, 96.60.Ly

Scientific paper

Local helioseismology techniques yielding the temperature and flow-velocity distributions under a sunspot indicate an unambiguous sign for the horizontal gas-pressure difference between the spot and ambient medium at depths of 4 Mm and more. In the Parker sunspot model, the transverse equilibrium condition cannot be satisfied in these layers: a cluster of vertical, strongly compressed magnetic flux tubes in a plasma that is hotter than the ambient medium with flows that diverge sidewise cannot be in equilibrium. Equilibrium can be satisfied in the hot zone under the spot only if the magnetic flux tube expands sharply with depth, so that the mean magnetic-field strength decreases dramatically at depths exceeding 4 Mm. This corresponds to the “shallow” sunspot model that has been used to interpret long-period sunspot oscillations.

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